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Relative directions of orbit or rotation
rotational axis. Prograde or direct motion is more normal motion in the same direction as the primary rotates. However, "retrograde" and "prograde" can also
Retrograde and prograde motion
Retrograde_and_prograde_motion
Apparent backward motion of a planet
vantage point. Direct motion or prograde motion is motion in the same direction as other bodies. While the terms direct and prograde are equivalent in this
Apparent_retrograde_motion
Topics referred to by the same term
Prograde can refer to: Retrograde and prograde motion, in astronomy, a type of motion of astronomical bodies Metamorphism#Prograde and retrograde, in
Prograde
Laws describing planetary orbits
In astronomy, Kepler's laws of planetary motion give good approximations for the orbits of planets around the Sun. They were published by Johannes Kepler
Kepler's laws of planetary motion
Kepler's_laws_of_planetary_motion
Type of spacecraft orbit
a distant retrograde orbit (DRO) is a highly stable retrograde orbit around the smaller of two bodies, passing outside the system's L1 and L2 Lagrange
Distant_retrograde_orbit
Angle between a reference plane and the plane of an orbit
the normal orbit is prograde, an orbit in the same direction as the planet rotates. Inclinations greater than 90° describe retrograde orbits (backward)
Orbital_inclination
Path on the surface of the Earth or another body directly below an aircraft or satellite
with an orbital inclination between zero and ninety degrees is said to be in what is called a direct or prograde orbit, meaning that it orbits in the same
Satellite_ground_track
Curved path of an object around a point
first order). A prograde or retrograde transverse impulse (i.e. an impulse applied along the orbital motion) changes both the eccentricity and the orbital
Orbit
Spacecraft end-of-life orbit
life to reduce the probability of colliding with operational spacecraft and generating space debris. A graveyard orbit is used when the change in velocity
Graveyard_orbit
Trajectory of Earth around the Sun
to the size of the orbit). As seen from Earth, the planet's orbital prograde motion makes the Sun appear to move with respect to other stars at a rate
Earth's_orbit
Earth). By convention, the inclination of a Prograde orbit is specified as an angle less than 90°. Retrograde orbit: An orbit counter to the direction of
List_of_orbits
Type of orbit around an astronomical body
plane of reference. The orbital inclination is 0° for prograde orbits, and π (180°) for retrograde ones.[citation needed] If the plane of reference is a
Near-equatorial_orbit
Table of positions of astronomical objects at given times
astronomers are eclipses, apparent retrograde motion/planetary stations, planetary ingresses, sidereal time, positions for the mean and true nodes of the moon, the
Ephemeris
Angular speed required for a body to complete one orbit
center of mass. While nominally a mean, and theoretically so in the case of two-body motion, in practice the mean motion is not typically an average over time
Mean_motion
Orbit keeping the satellite at a fixed longitude above the equator
over Australia. Geosynchronous satellites are launched to the east into a prograde orbit that matches the rotation rate of the equator. The smallest inclination
Geosynchronous_orbit
Parameters that define a specific orbit
equatorial orbits, and inclinations near 90° indicate polar orbits. Inclinations from 90 to 180° are typically used to denote retrograde orbits. Longitude
Orbital_elements
Type of orbit
with the eccentricity (e) equal to 1 and is an unbound orbit that is exactly on the border between elliptical and hyperbolic. When moving away from the
Parabolic_trajectory
Satellite orbit with high inclination
discovery was made with the help of radial velocity measurements that showed retrograde apsidal precession of the brown dwarf pair, which could not be explained
Polar_orbit
Geocentric orbit with an altitude entirely above that of a geosynchronous orbit
make groundbreaking discoveries in astronomy and Earth science, while also enabling global communication and navigation systems. The Moon's Hill sphere
High_Earth_orbit
System for specifying positions of celestial objects
.S. Poleski, Radosław (2013). "Transformation of the equatorial proper motion to the Galactic system". arXiv:1306.2945 [astro-ph.IM]. Wikimedia Commons
Astronomical coordinate systems
Astronomical_coordinate_systems
Region in which an astronomical body dominates the attraction of satellites
primary body, retrograde orbits remain stable over a wider region than prograde orbits. This was thought to explain the preponderance of retrograde moons around
Hill_sphere
Transfer orbit used to reach geosynchronous or geostationary orbit
Geostationary and geosynchronous orbits are very desirable for many communication and Earth observation satellites. However, the delta-v, and therefore financial
Geostationary_transfer_orbit
Classical approach to the many-body problem of astronomy
In astronomy, perturbation is the complex motion of a massive body subjected to forces other than the gravitational attraction of a single other massive
Perturbation_(astronomy)
Circular orbit above Earth's Equator and following the direction of Earth's rotation
operated by Fugro. Geostationary satellites are launched to the east into a prograde orbit that matches the rotation rate of the equator. The smallest inclination
Geostationary_orbit
Natural satellites of the planet Jupiter
outer irregular satellites whose prograde and retrograde orbits are much farther from Jupiter and have high inclinations and eccentricities. The largest of
Moons_of_Jupiter
Timekeeping system on Earth relative to the celestial sphere
day for retrograde rotation, as the rotation of the planet would be against the direction of orbital motion. If a planet rotates prograde, and the sidereal
Sidereal_time
Time an astronomical object takes to complete one orbit around another object
gravitational constant. In a parabolic or hyperbolic trajectory, the motion is not periodic, and the duration of the full trajectory is infinite. For celestial
Orbital_period
Natural satellites of the planet Neptune
Neptune has eight outer irregular satellites: four retrograde and four prograde. Among the prograde satellites is Nereid, the largest of the eight outer
Moons_of_Neptune
Either of two extreme points in a celestial object's orbit
are apogee and perigee. For the Sun, the suffix is -helion, so the names are aphelion and perihelion. According to Newton's laws of motion, all periodic
Apsis
Low-energy trajectories in the Solar System
trajectory will diverge away from the L1 point. The entire system is in motion, so the spacecraft will not actually hit the Moon, but will travel in a
Interplanetary Transport Network
Interplanetary_Transport_Network
Transfer manoeuvre between two orbits
geostationary orbit. In the idealized case, the initial and target orbits are both circular and coplanar. The maneuver is accomplished by placing the craft
Hohmann_transfer_orbit
Orbit in the two body case with high eccentricity
named after the Molniya Soviet communication satellites which used them, and Tundra orbits. Many US satellites also have used these orbits, satellites
Highly_elliptical_orbit
Type of orbital maneuver
Hohmann transfer requires 15 hours and 34 minutes. Δv applied prograde Δv applied retrograde Evidently, the bi-elliptic orbit spends more of its delta-v
Bi-elliptic_transfer
Range of low orbital altitudes
scenarios and for multiple applications, in both private and government satellite operations. Applications include Earth observation (especially gravity and magnetic
Very_low_Earth_orbit
Orbit of an object around the Moon
provide stable orbits in the lunar vicinity, such as halo orbits and distant retrograde orbits. Some halo orbits remain over particular regions of the lunar
Lunar_orbit
Natural satellites of the planet Uranus
highlighted in light blue and bolded. The inner and major moons all have prograde orbits. Irregular moons with retrograde orbits are shown in dark grey
Moons_of_Uranus
Orbit around Earth between 160 and 2000 km
inclination, allow rapid revisit times over low-latitude locations on Earth. Prograde equatorial LEOs also have lower delta-v launch requirements because they
Low_Earth_orbit
Highly elliptical and highly inclined synchronous orbit
inclination, e {\displaystyle e} is the eccentricity, n {\displaystyle n} is mean motion in degrees per day, J 2 {\displaystyle J_{2}} is the perturbing factor,
Tundra_orbit
Type of geocentric orbit
and inclinations of around 98°. This is slightly retrograde compared to the direction of Earth's rotation: 0° represents an equatorial orbit, and 90°
Sun-synchronous_orbit
Concept in astrodynamics
semi major axis and the eccentricity. However, with a hyperbolic orbit other parameters may be more useful in understanding a body's motion. The following
Hyperbolic_trajectory
Movement during spaceflight
be used to accelerate, decelerate and/or re-direct the path of a spacecraft. The "assist" is provided by the motion (orbital angular momentum) of the
Orbital_maneuver
Field of classical mechanics concerned with the motion of spacecraft
ballistics and celestial mechanics to rockets, satellites, and other spacecraft. The motion of these objects is usually calculated from laws of motion and of
Orbital_mechanics
Concept in celestial mechanics
trajectory – no other forces are acting on the object, such as propulsion and friction No other gravity-producing objects exist. Although the term escape
Escape_velocity
Mathematical equation describing the motion of a rocket
or ideal rocket equation is a mathematical equation that describes the motion of vehicles that follow the basic principle of a rocket: a device that can
Tsiolkovsky_rocket_equation
Time period during which a rocket must launch to reach its target
In the context of spaceflight, launch period is the collection of days, and launch window is the time period on a given day, during which a particular
Launch_window
Maintenance of a particular orbit
Earth's gravity field from that of a homogeneous sphere and gravitational forces from the Sun and Moon will in general perturb the orbital plane. For a
Orbital_station-keeping
Type of co-orbital motion of a small orbiting body relative to a larger orbiting body
horseshoe orbits and quasi-satellite orbits. Quasi-satellites aren't gravitationally bound to their planet, but appear to circle it in a retrograde direction
Horseshoe_orbit
Measure of amount of effort to change trajectory
known as "change in velocity"), symbolized as Δ v {\textstyle {\Delta v}} and pronounced /dɛltə viː/, as used in spacecraft flight dynamics, is a measure
Delta-v
Amount by which an orbit deviates from a perfect circle
circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabolic (escape orbit or capture orbit), and greater than 1 is a hyperbola. The
Orbital_eccentricity
Periodic, three-dimensional orbit
bodies and has nearly stable behavior. The CAPSTONE mission, launched in 2022, is the first spacecraft to use such orbit in cislunar space, and this Moon-centric
Near-rectilinear_halo_orbit
Movement around a celestial body that remains below its Karman line
usually due to a launch vehicle malfunction. Such satellites include EOS 02 and AzaadiSAT, which were deployed into a 76 km × 356 km (47 mi × 221 mi) transatmospheric
Transatmospheric_orbit
Specifies the orbit of an object in space
\right)~,} and here mean anomaly represents uniform angular motion on a circle of radius a. Mean anomaly can be calculated from the eccentricity and the true
Mean_anomaly
Earth-centered orbit above low Earth orbit and below geostationary orbit
orbit (LEO) and below a high Earth orbit (HEO) – between 2,000 and 35,786 km (1,243 and 22,236 mi) above sea level. The boundary between MEO and LEO is an
Medium_Earth_orbit
Problem in physics and celestial mechanics
a planet's motion; i.e., to give its orbital properties: position, orbital diameter, period and orbital velocity. Having done so, he and others soon
N-body_problem
Parameter of Keplerian orbits
Projective geometry Kepler's laws of planetary motion Ellipse Hyperbola Fundamentals of Astrodynamics and Applications by David A. Vallado Broucke, R.;
True_anomaly
Orbit around the barycenter of the Sun
in 2013. Astrodynamics – Field of classical mechanics concerned with the motion of spacecraftPages displaying short descriptions of redirect targets Earth's
Heliocentric_orbit
motion of a planet around the Sun, this position is called longitude of perihelion ϖ, which is the sum of the longitude of the ascending node Ω, and the
Longitude_of_periapsis
Branch of astronomy about the celestial sphere
Jyotish Kepler's laws of planetary motion Occultation Parallax Retrograde and prograde motion Sidereal time Solstice Robin M. Green, Spherical Astronomy,
Spherical_astronomy
Defining the orbit of an object in space
reference, as seen in the adjacent image. Commonly used reference planes and origins of longitude include: For geocentric orbits (e.g., artificial satellites
Longitude of the ascending node
Longitude_of_the_ascending_node
Kind of planetary orbit
than the sidereal day of the planet. An Earth satellite that is in (a prograde) subsynchronous orbit will appear to drift eastward as seen from the Earth's
Subsynchronous_orbit
Kepler orbit with an eccentricity of less than one
the Sun are ellipses with the Sun at one focus, and described this in his first law of planetary motion. Later, Isaac Newton explained this as a corollary
Elliptic_orbit
Spaceflight maneuver
mean motion a {\displaystyle a\,} is the semi-major axis For more complicated maneuvers which may involve a combination of change in inclination and orbital
Orbital_inclination_change
Equilibrium points near two orbiting bodies
exact centripetal force required to maintain the circular motion that matches their orbital motion. Alternatively, when seen in a rotating reference frame
Lagrange_point
Quasiperiodic orbit around a Lagrange point
quasiperiodic orbit around a Lagrange point. Libration is a form of orbital motion exhibited, for example, in the Earth–Moon system. Trojan bodies also exhibit
Libration_point_orbit
Orbital data format
time, the epoch. Using a suitable prediction formula, the state (position and velocity) at any point in the past or future can be estimated to some accuracy
Two-line_element_set
2010 British television series
Mountains, and relates how in clear night skies the ancients observed the rotation of the stars and the retrograde and prograde motion of Mars and the other
Wonders_of_the_Solar_System
Type of spacecraft maneuver
{\displaystyle W={\vec {F}}\cdot {\vec {s}}.} If the burn is made in the prograde direction, F → ⋅ s → = ‖ F ‖ ⋅ ‖ s ‖ = F ⋅ s {\displaystyle {\vec {F}}\cdot
Oberth_effect
Spacecraft launch or descent maneuver
without first going into lunar orbit. The vehicle begins by orienting for a retrograde burn to reduce its orbital velocity, lowering its point of periapsis to
Gravity_turn
Astrodynamic equation
or hyperbolic orbit): the motion is either away from the central body, or towards it. if the energy is negative: the motion can be first away from the
Orbit_equation
Quasi-periodic orbital trajectory
bodies. In contrast, Lissajous orbits are space curves and include components in this plane and perpendicular to it. Halo orbits also include components
Lissajous_orbit
Concept in celestial mechanics
{GMm}{r^{2}}}={\frac {\mu m}{r^{2}}}} Thus only the product of G and M is needed to predict the motion of the smaller body. Conversely, measurements of the smaller
Standard gravitational parameter
Standard_gravitational_parameter
Natural satellites of the planet Saturn
their orbital characteristics into the prograde Inuit and Gallic groups and the large retrograde Norse group, and their names are chosen from the corresponding
Moons_of_Saturn
Term in geometry; longest and shortest semidiameters of an ellipse
ellipse is its longest diameter: a line segment that runs through the center and both foci, with ends at the two most widely separated points of the perimeter
Semi-major and semi-minor axes
Semi-major_and_semi-minor_axes
The Moon's circuit around Earth
the prograde direction and completes one revolution relative to the Vernal Equinox and the fixed stars in about 27.3 days (a tropical month and a sidereal
Orbit_of_the_Moon
Globular cluster
The structure of the cluster is itself chaotic, with both retrograde and prograde motion observed in the movement of its stars. Low mass X-ray binary
Terzan_2
Parameter in the gravitational two-body problem
of their mutual potential energy, ε p {\displaystyle \varepsilon _{p}} , and their kinetic energy, ε k {\displaystyle \varepsilon _{k}} ) to their reduced
Specific_orbital_energy
Satellites of Jupiter
Jupiter, half of them prograde (Himalia, Elara, Lysithea, and Leda) and half of them retrograde (Pasiphae, Carme, Sinope, and Ananke). These eight are
Himalia_group
Moment in time used as a reference point in astronomy
this way is to calculate other relevant parameters of motion, in order to predict future positions and velocities. The applied tools of the disciplines of
Epoch_(astronomy)
Motion of Earth's rotational axis relative to its crust
is the sum of a prograde and a retrograde circular polarized wave. For frequencies ν < 0.9 the retrograde wave can be neglected, and there remains the
Polar_motion
Periodic, three-dimensional orbit
first computed in 1998 by M.A. Andreu, who introduced a new model for the motion of a spacecraft in the Earth-Moon-Sun system, which was called Quasi-Bicircular
Halo_orbit
Angle defining a position in an orbit
angle measured at the center of the ellipse between the orbit's periapsis and the current position. The eccentric anomaly is one of three angular parameters
Eccentric_anomaly
Celestial orbit whose trajectory is a conic section in the orbital plane
Keplerian orbit, named after the German astronomer Johannes Kepler) is the motion of one body relative to another, in the form of an ellipse, parabola, or
Kepler_orbit
Orbit with a fixed distance from the barycenter
in direction. If it is constant in magnitude and changing in direction with the velocity, circular motion ensues. Taking two derivatives of the particle's
Circular_orbit
Vector quantity in celestial mechanics
connects the two bodies. The proof starts with the two body equation of motion, derived from Newton's law of universal gravitation: r ¨ + G m 1 r 2 r r
Specific_angular_momentum
Characteristic of conic sections
of a circle is 0. The eccentricity of a non-circular ellipse is between 0 and 1. The eccentricity of a parabola is 1. The eccentricity of a hyperbola is
Eccentricity_(mathematics)
Temporary orbit used during the launch of a spacecraft
stage is fired to raise the spacecraft's apogee to geostationary altitude (and often reduce the inclination of the transfer orbit, as well). Finally, a
Parking_orbit
Complex type of orbit
than a point gravitational source, resulting in a non-closed orbit. A prograde relativistic shift happens because of relativistic effects from a massive
Rosetta_orbit
Circular areosynchronous orbit in the Martian equatorial plane
equator and following the direction of Mars's rotation. An object in such an orbit has an orbital period equal to Mars's rotational period, and so to ground
Areostationary_orbit
Specifies the orbit of an object in space
the body's ascending node to its periapsis, measured in the direction of motion. For specific types of orbits, terms such as argument of perihelion (for
Argument_of_periapsis
Kind of planetary orbit
high, and current public policy does not require nor incentivize rapid removal by the party that first inserted the debris in outer space and thus created
Supersynchronous_orbit
Space navigation technique
"assist" is provided by the motion of the gravitating body as it pulls on the spacecraft. Any gain or loss of kinetic energy and linear momentum by a passing
Gravity_assist
Orbital perturbations
celestial mechanical analyses of the motion have been carried out (as they have been for the major planets, the Moon, and other planetary satellites), the
Osculating_orbit
Orbit around Earth
could follow a parabolic capture trajectory, but speed and direction would have to be precise. Prograde orbit an orbit in which the projection of the object
Geocentric_orbit
Estimate of total change in velocity of a space mission
Because delta-v depends on the position and motion of celestial bodies, particularly when using the slingshot effect and Oberth effect, the delta-v budget changes
Delta-v_budget
is equatorial (in the same plane as the equator of Mars), circular, and prograde (rotating about Mars's axis in the same direction as the planet's surface)
Areosynchronous_orbit
Propulsive maneuver used to arrive at the Moon
sphere of influence. Motion in a patched-conic system is deterministic and simple to calculate, lending itself for rough mission design and "back of the envelope"
Trans-lunar_injection
Spaceflight where spacecraft orbits an astronomical body
with the center of the Earth, and may be inclined with respect to the equator. The relative motion of the spacecraft and the movement of the Earth's surface
Orbital_spaceflight
Speed at which a body orbits around the barycenter of a system
total energy is negative, Ek − Ep < 0: The orbit is bound, or closed. The motion will be on an ellipse with one focus at the other body. See radial elliptic
Orbital_speed
Type of high-latitude satellite orbit
inclination, e {\displaystyle e} is the eccentricity, n {\displaystyle n} is mean motion in degrees per day, J 2 {\displaystyle J_{2}} is the perturbing factor,
Molniya_orbit
change in position within the orbit is usually defined as the phase angle, ϕ, and is the change in true anomaly required between the spacecraft's current position
Orbit_phasing
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